We have derived elemental abundances of O , Na , Mg , Al , Si , Ca , Ti , Cr , Mn , Fe , Co , Ni as well as for a number of s-elements for 47 G and K dwarf , with [ Me/H ] > 0.1 dex .
The selection of stars was based on their kinematics as well as on their uvby - \beta -photometry .
One sample of stars on rather eccentric orbits traces the chemical evolution interior to the solar orbit and another , on circular orbits , the evolution around the solar orbit .
A few Extreme Population I stars were included in the latter sample .

The stars have -0.1 dex < { [ Fe / H ] } < 0.42 dex .
The spectroscopic [ Fe/H ] correlate well with the [ Me/H ] derived from uvby - \beta photometry .
We find that the elemental abundances of Mg , Al , Si , Ca , Ti , Cr and Ni all follow [ Fe/H ] .
Our data put further constraints on models of galactic chemical evolution , in particular of Cr , Mn and Co which has not previously been studied for dwarf stars with { [ Me / H ] } > 0.1 dex .
The increase in [ Na/Fe ] and [ Al/Fe ] as a function of [ Fe/H ] found previously by Edvardsson et al .
( 1993a ) has been confirmed for [ Na/Fe ] .
This upturning relation , and the scatter around it , are shown not to be due to a mixture of populations with different mean distances to the galactic centre .
We do not confirm the same trend for aluminium , which is somewhat surprising since both these elements are thought to be produced in the same environments in the pre-supernova stars .
Nor have we been able to trace any tendency for relative abundances of O , Si , and Ti relative to Fe to vary with the stellar velocities , i.e .
the stars present mean distance to the galactic centre .
These results imply that there is no significant difference in the chemical evolution of the different stellar populations for stars with [ Me/H ] > 0.1 dex .
We find that [ O/Fe ] continue to decline with increasing [ Fe/H ] and that oxygen and europium correlate well .
However [ Si/Fe ] and [ Ca/Fe ] seem to stay constant .
A real ( ” cosmic ” ) scatter in [ Ti/Fe ] at given [ Fe/H ] is suggested as well as a decreasing abundance of the s-elements relative to iron for the most metal-rich dwarf stars .
We discuss our results in the context of recent models of galactic chemical evolution .

In our sample we have included a few very metal rich stars , sometimes called SMR ( super metal rich ) stars .
We find these stars to be among the most iron-rich in our sample but far from as metal-rich as indicated by their photometric metallicities .
SMR stars on highly eccentric orbits , alleged to trace the evolution of the chemical evolution in the galactic Bulge , have previously been found overabundant in O , Mg and Si .
We have included three such stars from the study by Barbuy & Grenon ( 1990 ) .
We find them to be less metal rich and the other elemental abundances remain puzzling .

Detailed spectroscopic abundance analyses of K dwarf stars are rare .
Our study includes 5 K dwarf stars and has revealed what appears to be a striking example of overionization .
The overionization is especially prominent for Ca , Cr and Fe .
The origin of this apparent overionization is not clear and we discuss different explanations in some detail .